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Annexe I : Description Des Services D’Observations Labellisés Liés À La Planétologie

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Annexe I : Description Des Services D’Observations Labellisés Liés À La Planétologie Annexe I : description des services d’observations labellisés liés à la planétologie Consultation BDD Service des éphémérides Type AA-ANO1 Coordination Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO IMCCE Jacques LASKAR Jacques LASKAR [email protected] Partenaires Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU Obs. Paris Claude CATALA OCA Thierry LANZ Agnès FIENGA [email protected] Description L'IMCCE a la responsabilité, sous l'égide du Bureau des longitudes, de produire et de diffuser les calendriers et éphémérides au niveau national. Cette fonction est assurée l'institut par son Service des éphémérides. Aussi celui-ci a) produit les publications et éditions annuelles tout comme les éphémérides en ligne, b) diffuse les éphémérides de divers corps du système solaire - naturels et artificiels, et de phénomènes célestes, c) assure la maintenance et la mise jour des bases de données, d) procure une expertise juridique aux tribunaux, e) procure des éphémérides et données la demande pour les services similaires (USA, Japon), les agences, les chercheurs, les laboratoires et les observatoires. Consultation BDD Gaia Type AA-ANO1, AA-ANO4 Coordination Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO OCA Thierry LANZ François MIGNARD [email protected] Partenaires Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU Obs. Paris Claude CATALA Frédéric ARENOU [email protected] IMCCE Jacques LASKAR Daniel HESTROFFER [email protected] OASU Marie Lise DUBERNET-TUCKEY Caroline SOUBIRAN [email protected] THETA Philippe ROUSSELOT Annie ROBIN [email protected] IAP Francis BERNARDEAU Brigitte ROCCA VOLMERANGE [email protected] ObAS Pierre-Alain DUC Jean-Louis HALBWACHS [email protected] Description Participation aux activités du Consortium DPAC (Data Processing and Analysis Consortium) pour la mission Gaia. Ceci comprend (i) la conception, la réalisation, la qualification et l'exécution des chaînes de traitement des données brutes du satellite devant aboutir la publication des produits Gaia, (ii) la validation des résultats et la production de l'ensemble de la documentation pour les utilisateurs chaque nouvelle remise de données (iii) la collecte d'informations complémentaires, nécessaires l'accomplissement de la mission, partir d'observations au sol. Consultation BDD CHARA Type AA-ANO2 Coordination Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO OCA Thierry LANZ Denis MOURARD [email protected] Partenaires Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU OSUG Michel DIETRICH Karine PERRAUT [email protected] OSUL Isabelle DANIEL Isabelle TALLON-BOSC [email protected] Obs. Paris Claude CATALA Vincent COUDE DU FORESTO [email protected] Description Ce service a pour objectif le soutien aux groupes français exploitant l'interféromètre du Center for High Angular Resolution Astronomy (CHARA, USA). Ce réseau interférométrique optique situé l'observatoire du Mount Wilson (Californie) comprend 6 télescopes de 1 mètre sur des bases allant de 30 330 mètres, et est équipé de 2 instruments français: JOUFLU pour la recombinaison très haute précision dans l'infrarouge proche (bande K), et VEGA pour l'imagerie interférométrique dans le visible haute résolution spectrale et très haute résolution spatiale. D'autres instruments sont également en service: MIRC (pour l'imagerie interférométrique en bandes H et K, Université de Michigan), CLASSIC-CLIMB (pour une sensibilité maximale en bandes H et K, Chara Center), et PAVO un instrument 3T dans le visible pour la haute sensibilité (Université de Sydney). L’accès CHARA et donc l’hémisphère Nord ainsi qu’au domaine du visible est un atout très intéressant et complémentaire du VLTI. Le soutien du service passe explicitement par les actions suivantes : 1) Soutien la préparation des observations et formation 2) Prise en charge des observations en mode service (dans le cadre de l’optimisation des nuits d’observation) et formation 3) Prise en charge/Soutien la réduction des données. Formation. 4) Maintenance technique, évolutions Sur ce dernier point, l'équipe VEGA Nice a développé un prototype appelé FRIEND destiné comprendre le fonctionnement en interférométrie visible avec une correction partielle par optique adaptative sur chacun des télescopes de 1m. Ce prototype prépare le développement de l'instrument SPICA (recombinaison visible 6T fibrée). Consultation BDD E-ELT / HARMONI Type AA-ANO2 Coordination Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO OSUL Isabelle DANIEL Roland BACON [email protected] Partenaires Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU PYTHEAS Bruno HAMELIN Benoit NEICHEL [email protected] Description Le spectrographe HARMONI est un des deux instruments de première lumière financés pour l’ELT européen. Il s’agit d’un spectrographe intégral de champ (IFU) qui observera dans la gamme visible et proche infra-rouge (de 0.5 2.4 microns). HARMONI fournira une résolution spectrale de R=3000 R=20000, et une résolution angulaire de 60 4 mas. Pour exploiter pleinement la limite de diffraction de l’E-ELT, HARMONI sera équipé de deux systèmes d’Optique Adaptative (OA). Le premier est un système d’OA classique (SCAO) et le deuxième sera un système d’OA grand champ, assisté par étoiles lasers (LTAO). HARMONI s’inscrit dans la lignée d’instruments qui équipent le VLT, tels que SPHERE ou MUSE. La première lumière est prévue pour 2024. Les cas scientifiques principaux d’HARMONI couvrent un large spectre, depuis l’étude et la caractérisation des exo-planètes, l’étude des populations stellaire dans les galaxies proches, et jusqu’aux galaxies grand décalage vers le rouge. HARMONI regroupe un consortium de 6 laboratoires, dont 2 laboratoires français : le LAM et le CRAL. Le CRAL réalise les modules de découpage du champ et les optiques relai, le pipeline de réduction des données, et (avec l’IPAG), le contrôle de l’instrument. Un modèle numérique de l’instrument (INM) est en développement au CRAL pour simuler des données brutes HARMONI et tester les différentes étapes de réduction en lien avec les développements du pipeline. Le LAM est en charge du développement des Optiques Adaptatives. Avec le LAM, l’IPAG est en charge du développement d’un bras d’imagerie haut-contraste permettant la caractérisation d’exoplanètes. Les tâches de services proposées au CRAL sont les suivantes : T1- Préparation de cas scientifiques clé pour tester le pipeline: Il s'agit d'extraire, partir de simulations astrophysiques ou d'observations existantes, des cas types d'observations simuler avec l'INM dans les principaux modes d'HARMONI (champs stellaires, galaxies, champs profonds), ainsi que des cibles spécifiques (cibles mouvantes, champs astrométriques). Ces données simulées serviront de test pour la réduction des données avec le pipeline. Ces résultats de réduction seront par ailleurs contrôlés dans une étape de validation par rapport aux données en entrée de l'INM, avec une quantification des erreurs et une étude de l'impact sur la science. T2- Proposition et validation d’algorithmes avancés pour les particularités d’HARMONI: Il s'agit de contribuer la réflexion sur les choix d'algorithmes, puis leur validation, concernant les calibrations basées sur des observations du ciel: l'astrométrie, la correction des telluriques, et la soustraction optimale du ciel. En particulier, nous projetons d'utiliser le mode multi-lectures pour les détecteurs: il faudra exploiter cette possibilité de manière optimale pour les algorithmes ci-dessus. T3- Participation au choix des tests de validation du pipeline qui seront effectuer en laboratoire et/ou sur le ciel au cours des phases de tests globaux puis de commissioning de l'instrument. Les tâches de services proposées au LAM sont : - Spécifications scientifiques de haut niveau et estimation de performances de l’instrument et des systèmes d’optique adaptative associés (SCAO et LTAO) sur la base des cas scientifiques prioritaires (formation et évolution des galaxies, formation stellaire, système solaire, exo-planètes, etc.) Ce travail inclut des activités de modélisation et/ou de simulation. Participation aux études systèmes, participation aux équipes scientifiques et techniques. - Spécification et préparation des logiciels d’acquisition et de réduction des données. Ce travail peut inclure des activités de démonstration et/ou de prototypage en laboratoire ou avec des démonstrateurs. Ces tâches devront évoluer au cours du cycle de développement de l’instrument vers des tâches de spécifications et d’étude de performance des sous-systèmes, puis de modélisation fine de ceux-ci, et enfin de caractérisation et de validation au cours des phases d’intégration et de tests puis de commissioning sur le ciel. Les tâches de services proposées l’IPAG, sont : - Les spécifications scientifiques de haut niveau et l’estimation des performances du bras haut-contraste sur la base des cas scientifiques prioritaires (caractérisation d’exoplanètes, étude des disques de formation, etc.). Ce travail inclut des activités de modélisation et/ou de simulation ainsi qu’une participation aux études systèmes. - La préparation des outils de réduction des données : outils classiques d’imagerie différentielle & outils innovants exploitant la haute résolution spectrale de HARMONI pour détecter des signatures spectrales de diverses molécules. Ces tâches devront évoluer au cours du cycle de développement de l’instrument vers des tâches de spécifications et d’étude de performance du bras haut-contraste, puis de modélisation fine de celui-ci, et enfin de caractérisation et de validation au cours des phases d’intégration et de tests puis de commissioning sur le ciel. Consultation BDD E-ELT / MICADO Type AA-ANO2 Coordination Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO Obs.
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